Presentation is loading. Please wait.

Presentation is loading. Please wait.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Published byLillian Matthews Modified over 8 years ago

Similar presentations

Presentation on theme: "Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION."— Presentation transcript:

1 Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION NUMBER ”. --- (The last 4 digits of your OleMiss ID.) Question # 1: answer A Question # 2: answer C Question # 3: answer C Setup: Please take a moment to mute your cell phone! Use a pencil, not a pen! Reading assignment Chapter 15, pp. 486-510 (Stars)

2 sec 30 Question 4 29 The spectra of stars normally are A emission spectrum: a few bright lines only. B absorption spectrum: dark lines over a bright continuum. C composite spectra: dark bands of light with bright centers, over a bright continuum. D continuous spectra: continuous bright spectrum like a rainbow. E molecular emission spectra: many wide, bright bands. 282726252423222120 19 181716151413121110 9 8 7 6 5 4 3 2 1 0 Next question coming … This question counts double!

3 sec 45 Question 5 403530252019181716151413121110 9 8 7 6 5 4 3 2 1 0 Next question coming … What is the Doppler effect? A Stars move on tiny circles in the sky, once a year. B A fast moving star ’ s spectral lines are redshifted, independently of the direction of motion. C Stars close to the center of the Galaxy appear red because the Universe is expanding. D The spectral lines of a star are shifted towards red, if the star is moving away from us, and towards blue, if the star is approaching us. E A star appears red when rising or setting. This question counts double!

4 sec 30 Question 6 29 The strongest line in the solar spectrum is a calcium line. Why is that? A The most abundant element in the solar photosphere is calcium. B Although the main constituent of the photosphere is hydrogen, there are dark calcium clouds floating higher up. C It is very easy for calcium, a metal, to have its electrons moved to an upper orbit. 282726252423222120 19 181716151413121110 9 8 7 6 5 4 3 2 1 0 This question counts double!

5 Spectroscopic binaries Calculate: * Orbital speed ( shift in % of wavelength = speed in % of speed of light ) * Size of orbit ( time period × speed = 2 r  ) Mass * Mass of stars ( Kepler III: M × T 2 = r 3 ) Measure: * Blue/red shift of lines * Time period Earth

6 Questions coming …

7 sec 30 Question 7 29 How do we know the mass of (some) stars? A Using measurements of their planets. B Using measurements of the force of their gravity on spaceships. C Using the red/blue shift of spectral lines of double stars. D Using measurements of their brightness and color. 282726252423222120 19 181716151413121110 9 8 7 6 5 4 3 2 1 0 Next question coming …

8 sec 45 Question 8 403530252019181716151413121110 9 8 7 6 5 4 3 2 1 0 In a star ’ s spectrum all the hydrogen lines are shifted towards red, and all the metal (sodium, calcium, etc. ) lines are blueshifted. This could be explained by the following situation: A The hydrogen in the star ’ s atmosphere is hotter than the metals. B The hydrogen in the star ’ s atmosphere is colder than the metals. C The star is a double, consisting of a regular star A plus a metal- reach star B. Star A is moving away from us, star B is approaching us as they revolve. D The star is a double, consisting of a regular star A plus a metal- reach star B. Star B is moving away from us, star A is approaching us as they revolve.

Download ppt "Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION."

Similar presentations

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.
Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.
Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.
Spectroscopy: and finding out the elements of deep space objects.

Spectroscopy: and finding out the elements of deep space objects.
Pre-Lecture Quiz: – MasteringAstronomy Ch15 pre-lecture quiz due February 17 – MasteringAstronomy Ch16 pre-lecture.

Pre-Lecture Quiz: – MasteringAstronomy Ch15 pre-lecture quiz due February 17 – MasteringAstronomy Ch16 pre-lecture.
Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.
Question 1 1) proton 2) electron 3) neutron 4) atomic nucleus

Question 1 1) proton 2) electron 3) neutron 4) atomic nucleus
Star Properties studied so far… Period Mass Eccentricity Red shift Velocity Temperature (Wiens Law) Composition – which elements and how much of each Color.

Star Properties studied so far… Period Mass Eccentricity Red shift Velocity Temperature (Wiens Law) Composition – which elements and how much of each Color.
< BackNext >PreviewMain Section 1 Stars Chapter 15 Bellringer List ways that stars differ from one another. How is the sun like other stars? How is it.

< BackNext >PreviewMain Section 1 Stars Chapter 15 Bellringer List ways that stars differ from one another. How is the sun like other stars? How is it.
Learning from Light Our goals for learning What are the three basic types of spectra? How does light tell us what things are made of? How does light tell.

Learning from Light Our goals for learning What are the three basic types of spectra? How does light tell us what things are made of? How does light tell.
Stars and Galaxies 28.1 A Closer Look at Light Chapter 28.

Stars and Galaxies 28.1 A Closer Look at Light Chapter 28.
PG. 127 Measuring the Stars. Groups of stars Long ago, people grouped bright stars and named them after animals, mythological characters or every day.

PG. 127 Measuring the Stars. Groups of stars Long ago, people grouped bright stars and named them after animals, mythological characters or every day.
Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.

Prepare your scantron: Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “ IDENTIFICATION.
Chapter 29 Notes Stars. The Sun: Solar Atmosphere Photoshere: visible surface, 5800 K Chromosphere: 30,000 K Corona: 1 to 2 million K, solar wind.

Chapter 29 Notes Stars. The Sun: Solar Atmosphere Photoshere: visible surface, 5800 K Chromosphere: 30,000 K Corona: 1 to 2 million K, solar wind.
What Can Spectroscopy Tell Us?. Atom or Molecular Fingerprints Every atom or molecule exists in its own unique energy state. This energy state is dependent.

What Can Spectroscopy Tell Us?. Atom or Molecular Fingerprints Every atom or molecule exists in its own unique energy state. This energy state is dependent.
Spectra  Chemistry and Doppler Effect Lecture 10.

Spectra  Chemistry and Doppler Effect Lecture 10.
Lecture 9 Stellar Spectra

Lecture 9 Stellar Spectra
Why is Light so useful in Astronomy? It can tell us many properties of planets and stars: –How warm / hot they are (Surface temperature) –What they’re.

Why is Light so useful in Astronomy? It can tell us many properties of planets and stars: –How warm / hot they are (Surface temperature) –What they’re.
Chapter 5 Light: The Cosmic Messenger. 5.2 Learning from Light Our goals for learning What types of light spectra can we observe? How does light tell.

Chapter 5 Light: The Cosmic Messenger. 5.2 Learning from Light Our goals for learning What types of light spectra can we observe? How does light tell.
PHYS1142 17 More about Electromagnetic Radiation Speed of light = frequency  wavelength = a constant c Q. How do we generate light? A. Heat things up.

PHYS More about Electromagnetic Radiation Speed of light = frequency  wavelength = a constant c Q. How do we generate light? A. Heat things up.

Similar presentations

Ads by Google